COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1320


                                      Konkoly Observatory
                                      Budapest
                                      1977 August 10


          ON THE VARIABLE STAR UU SAGITTAE



   This eclipsing star has been studied by Bezdenezhny and
Tsessevich (1) and the following elements have been obtained
       Min.hel.JD = 2432797.283 + 0.4650697 E.     (A)
   Recently Bond (2) has discovered that this star is the 
nucleus of a planetary nebula which makes it distinguished among
all the other objects. Muller, Krzeminski and Priedhorsky (3)
confirmed the eclipsing character of light variation independently 
of us and determined nearly the same value of the period.
They also reported the moment of the minimum observed which I
have taken into account when I have improved the period evaluated 
by me.
   Since the time my book (1) was published, more and more sky
photographs of Moscow collections have been gained. From these

          Moments of minima of UU Sagittae

     Min.hel.JD      E    O-C     Source of
                                 Information

     2432797.283      0   +0.003    Simeis
        3033.534    508   - .002      "
        3447.439   1398   - .009      "
        3448.379   1400   + .001      "
        7163.358   9388   + .006    Moscow
        7176.381   9416   + .007      "
       40512.310  16589   - .007       "
        0819.266  17249   + .003       "
        1475.468  18660   - .008       "
        1564.312  18851   + .007       "
        2626.520! 21135   - .003       "
        3013.928  21968   + .002     IAU Circ.2974

new observations a mean light curve (Fig. 1) and a moment of 
minimum have been obtained by me. All the known moments are given
in the table; the O-C residuals are calculated with the new 
improved formula:
  Min.hel.JD = 2432797.2805+0.46506944 E; P-1=2.1502165. (B)

                     [FIGURE 1-2]

    In Figure 2 observations ranging from phases -0.1p to +0.1p
reduced to one period with the formula (B) are shown. As is seen
from Figure 2 the light curve undergoes essential fluctuations
which are not unexpected.




                                  V.P. TSESSEVICH
                                Odessa Astronomical
                                   Observatory
                                     U.S.S.R.




References:
1 Tsessevich, V.P., "Studies of Variable Stars in Selected
          Regions of the Galactic Field", Kiev
2 Bond, H.E., PASP, No. 522, 192 [BIBCODE 1976PASP...88..192B ]
3 Miller, J.S., Krzeminski, W., Priedhorsky, IAU Circular 2974 [BIBCODE 1976IAUC.2974R...1M ]